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Interstellar Dust in the Solar System

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Abstract

Interstellar dust from the Local Interstellar Cloud was detected unambiguously for the first time in 1992 (Grün et al. in Nature 362:428–430, 1993). Since then, great progress has been made in observing local interstellar dust in the Solar System using a variety of methods that, all together, provide complementary views of the dust particles from our local galactic neighborhood. The complementary methods discussed in this paper are: (1) in situ observations with dust detectors, (2) sample return, (3) observations of dust in the infrared, and (4) detections using spacecraft antennae. We review the current state of the art of local interstellar dust research, with a special focus on the advances made in the last ∼10 years of interstellar dust research. We introduce this paper with an overview of the definitions of interstellar dust. We describe the dynamics of the dust particles moving through the heliosphere and report on the progress made in the modelling efforts especially in the last decade. We also review the currently available in situ measurements of interstellar dust flux, speed, direction and size distribution from various missions, in specific from Ulysses and Cassini, and their interpretation in context of the dust dynamics studies. Interstellar dust composition is also reviewed from Cassini in situ time of flight measurements and from the Stardust sample return mission that both took place in the last decade. Finally, also new dust measurements from spacecraft antennae are reviewed. The paper concludes with a discussion on currently still open questions, and an outlook for the future.

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Notes

  1. The Local Interstellar Cloud is a warm, low-density cloud surrounding the solar system that is located itself in a hot and even lower-density region called the “Local Bubble” (Frisch et al. 2011).

  2. The heliosphere is the region of space around the Sun that is dominated by the solar wind plasma, with respect to the ISM plasma.

  3. This contemporary extrasolar dust may be modified by its journey through the solar system and near the Sun though.

  4. See Schwehm (1976) and Burns et al. (1979) for calculating radiation pressure efficiencies, and Silsbee and Draine (2016) and Kimura (2017) for a discussion on the radiation pressure efficiencies for ISD, applied in specific to the Stardust mission (Sect. 5).

  5. A newer analysis of the complete Ulysses dataset, but excluding the period where the dust flow was shifted in direction (2005, see Sect. 3.2), has resulted in a derived flow direction of \(+75^{\circ }\pm 30\) ecliptic longitude and \(-13^{\circ }\pm 4\) ecliptic latitude (Strub et al. 2015). This corresponds roughly to the flow direction of the interstellar helium from IBEX He data between 2009 and 2013: \(+75.6^{\circ }\pm 1.4\) ecliptic longitude, and \(-5.12^{\circ }\pm 0.27\) ecliptic latitude (Schwadron et al. 2015) and earlier ISD directions derived from Ulysses data by Landgraf (1998), Frisch et al. (1999), and Kimura et al. (2003b). The average speed of the ISD particles measured by Ulysses was \(24\pm 12~\mbox{km}\,\mbox{s}^{-1}\) (Krüger et al. 2015), compatible with the Helium inflow speed of \(26.3\pm 0.4~\mbox{km}\,\mbox{s}^{-1}\) (Witte 2004) and with earlier determination of the heliocentric ISD inflow speed \(V_{\infty ,\mathit{ISD}} = 25.7\pm 0.5~\mbox{km}\,\mbox{s}^{-1}\) from the then available Ulysses ISD data by Kimura et al. (2003b).

  6. See Sterken et al. (2013) for examples of gravitational focusing effects for \(\beta =0.5\) at Asteroid, Jupiter and Saturn distance from the Sun, in the ecliptic plane.

  7. Mukai (1981) calculated an equilibrium potential of \(+0.5\) to \(+6~\mbox{V}\) for graphite at 1 AU and \(+4\) to \(+14~\mbox{V}\) for silicate grains depending on solar wind conditions. For charging in other plasma conditions (e.g. in the heliosphere boundary regions), we refer to Sect. 2.2.

  8. Figures 45 and 46 in Sterken et al. (2012) visualize such “Lorentz-force-modulated \(\beta \)-cones”.

  9. Kimura and Mann (1998) found \(+12~\mbox{V}\) for Silicate particles and \(+6~\mbox{V}\) for Carbon for particles with radius about 0.3 μm, while Alexashov et al. (2016) estimated a potential of \(+2\) to \(+3~\mbox{V}\). Ma et al. (2013) calculated higher charges for aggregates than for compact spheres (see Sect. 2.1.2)

  10. The inner heliosphere is the part of the heliosphere where the solar wind dominates the plasma and is still supersonic.

  11. Figure 19 in Sterken et al. (2015) illustrates how the incoming particles move through a different phase of the solar cycle in the solar system than they did earlier when crossing the heliosphere boundary regions.

  12. The heliopause is the boundary between the solar wind dominated inner heliosphere, and the region around the heliosphere where interstellar medium plasma dominates.

  13. ISD data from Helios were sampled between 1974 and 1980, before Ulysses, but were recognized in the data and analysed only after the first Ulysses ISD detections (Altobelli 2004; Altobelli et al. 2006).

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Acknowledgements

FP received financial support from the German Research Foundation (DFG) projects PO 1015/3-1, /4-1, and ERC Consolidator Grant 724908-Habitat OASIS.

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Authors and Affiliations

  1. Astronomisches Institut Universität Bern (AIUB), Bern, Switzerland

    Veerle J. Sterken

  2. Institute of Applied Physics (IAP), University of Bern, Bern, Switzerland

    Veerle J. Sterken

  3. Space Sciences Laboratory, University of California at Berkeley, Berkeley, USA

    Andrew J. Westphal

  4. European Space Agency, ESAC, Madrid, Spain

    Nicolas Altobelli

  5. LASP, University of Colorado, Boulder, USA

    David Malaspina

  6. Institute of Earth Sciences, University of Heidelberg, Heidelberg, Germany

    Frank Postberg

  7. Institute of Geological Sciences, Freie Universität Berlin, Berlin, Germany

    Frank Postberg

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Cosmic Dust from the Laboratory to the Stars

Edited by Rafael Rodrigo, Jürgen Blum, Hsiang-Wen Hsu, Detlef Koschny, Anny-Chantal Levasseur-Regourd, Jesús Martín-Pintado, Veerle Sterken and Andrew Westphal

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Sterken, V.J., Westphal, A.J., Altobelli, N. et al. Interstellar Dust in the Solar System. Space Sci Rev 215, 43 (2019). https://doi.org/10.1007/s11214-019-0607-9

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